Observational evidence that massive cluster galaxies were forming stars at<i>z</i>~ 2.5 and did not grow in mass at later times

Andreon, S.

doi:10.1051/0004-6361/201321071

Cited by 27 publications

(24 citation statements)

References 62 publications

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“…Our result is consistent with the conclusions drawn in Andreon (2013), which suggest that mass build-up in massive cluster galaxies is mostly complete by z 1.8…”

Section: Discussionsupporting

confidence: 93%

Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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We compile a sample of spectroscopically and photometrically selected cluster galaxies from four high-redshift galaxy clusters ( z 1.59 1.71 < <) from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS), and a comparison field sample selected from the UKIDSS Deep Survey. Using near-infrared imaging from the Hubble Space Telescope, we classify potential mergers involving massive (M M 3 10 10 * ´) cluster members by eye, based on morphological properties such as tidal distortions, double nuclei, and projected near neighbors within 20 kpc. With a catalog of 23 spectroscopic and 32 photometric massive cluster members across the four clusters and 65 spectroscopic and 26 photometric comparable field galaxies, we find that after taking into account contamination from interlopers, 11.0 % 5.6 7.0 -+ of the cluster members are involved in potential mergers, compared to 24.7 % 4.6 5.3 -+ of the field galaxies. We see no evidence of merger enhancement in the central cluster environment with respect to the field, suggesting that galaxy-galaxy merging is not a stronger source of galaxy evolution in cluster environments compared to the field at these redshifts.

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“…Our result is consistent with the conclusions drawn in Andreon (2013), which suggest that mass build-up in massive cluster galaxies is mostly complete by z 1.8…”

Section: Discussionsupporting

confidence: 93%

Galaxy Merger Candidates in High-redshift Cluster Environments

Delahaye

Webb

Nantais

et al. 2017

ApJ

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“…Saracco, Longhetti & Andreon 2009;Williams et al 2010;Poggianti et al 2013; but see Trujillo, Ferreras &de la Rosa 2011 andAndreon 2013). If this dependence is true, it implies that the selected galaxies will be the most compact ones, posing a strong selection bias when comparing to a local population.…”

Section: Introductionmentioning

confidence: 99%

“…It is assumed that the cluster ETGs are largely passively evolving since at least z∼ 1.2 (e.g. Andreon 2008;de Propris, Phillipps & Bremer 2013), with its red-sequence being already in place at even higher redshifts (e.g. Bower, Lucey & Ellis 1992, Kodama & Arimoto 1997Blakeslee et al 2003;de Lucia et al 2007;Faber et al 2007) and showing no significant evolution on the Fundamental Plane (e.g.…”

Section: Introductionmentioning

confidence: 99%

A TALE OF A RICH CLUSTER ATz∼ 0.8 AS SEEN BY THE STAR FORMATION HISTORIES OF ITS EARLY-TYPE GALAXIES

Ferré-Mateu¹,

Sánchez‐Blázquez

Vazdekis

et al. 2014

ApJ

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We present a detailed stellar population analysis for a sample of 24 early-type galaxies belonging to the rich cluster RX J0152.7-1357 at z = 0.83. We have derived the age, metallicity, abundance pattern and star formation history for each galaxy individually, to further characterize this intermediate-z reference cluster. We then study how these stellar population parameters depend on local environment. This provides a better understanding on the formation timescales and subsequent evolution of the substructures in this cluster. We have also explored the evolutionary link between z∼0.8 ETGs and those in the local Universe by comparing the trends that the stellar population parameters follow with galaxy velocity dispersion at each epoch. We find that the ETGs in Coma are consistent with being the (passively-evolving) descendants of the ETG population in RXJ10152.7-1357. Furthermore, our results favor a downsizing picture, where the subclumps centers were formed first. This central parts contain the most massive galaxies, which formed the bulk of their stars in a short, burst-like event at high-z. On the contrary, the cluster outskirts are populated with less massive, smaller galaxies, which show a wider variety of Star Formation Histories. In general, they present extended star formation episodes over cosmic time, which seems to be related to their posterior incorporation into the cluster, around 4 Gyr later after the initial event of formation.

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“…Indeed, cluster cores in the nearby Universe host the most massive early-type galaxies, containing stars nearly as old as the Universe, and producing the tight red sequence in the colormagnitude diagram of cluster galaxies (Visvanathan & Sandage 1977;Bower et al 1992;Kodama & Arimoto 1997) that is often considered to be a defining signature of high-density environments at low and intermediate redshifts. Most studies of the evolution of the red sequence and of the cluster galaxy luminosity function up to z ∼ 1−1.3 largely agree on a broad-brush picture where the high-mass end of the cluster galaxy population is largely in place even before redshift one, with the bulk of its stars formed in a massive star formation event in the cluster progenitor environments at z ∼ 2 or higher (e.g., De Propris et al 1999Propris et al , 2007Andreon 2006Andreon , 2013Strazzullo et al 2006Strazzullo et al , 2010Lin et al 2006;Lidman et al 2008;Mei et al 2009;Mancone et al 2010;Wylezalek et al 2014;Foltz et al 2015), followed by efficient suppression of star formation in a major part of the massive galaxy population, creating a first red sequence (e.g., Kodama et al 2007;Zirm et al 2008;Strazzullo et al 2016). Direct observations of the star formation suppression in high-redshift clusters add important constraints to this broad-brush picture (e.g., Muzzin et al 2014;Balogh et al 2016;Noble et al 2016;Rudnick et al 2017) concerning time scales, relevance, and actual nature of environmental effects (e.g., Wetzel et al 2012Wetzel et al , 2013Hirschmann et al 2014;Bahé et al 2017, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Galaxy populations in the most distant SPT-SZ clusters

Strazzullo

Pannella

Mohr

et al. 2019

A&A

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We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg2 South Pole Telescope Sunyaev Zel’dovich effect (SPT-SZ) survey, which is sensitive to M500 ≳ 3 × 1014 M⊙ clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z ≳ 1.4, S/NSZE > 5 clusters, that are among the rarest most massive clusters known at this redshift. All five clusters show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates, although one (SPT-CLJ0607–4448) shows a galaxy concentration much less prominent than the others. The highest redshift cluster in this sample, SPT-CLJ0459–4947 at z ∼ 1.72, is the most distant M500 > 1014 M⊙ cluster discovered thus far through its intracluster medium, and is one of only three known clusters in this mass range at z ≳ 1.7, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, we find that the quiescent fraction in the cluster central regions (r/r500 < 0.7) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range ∼0.5 − 0.8 for stellar masses log(M/M⊙) > 10.85. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/NSZE> 5, even if they had the same quiescent fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in the central regions of the most massive clusters, occurring already earlier than z ∼ 1.5.

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Observational evidence that massive cluster galaxies were forming stars atz~ 2.5 and did not grow in mass at later times

Cited by 27 publications

References 62 publications

Galaxy Merger Candidates in High-redshift Cluster Environments

Galaxy Merger Candidates in High-redshift Cluster Environments

A TALE OF A RICH CLUSTER ATz∼ 0.8 AS SEEN BY THE STAR FORMATION HISTORIES OF ITS EARLY-TYPE GALAXIES

Galaxy populations in the most distant SPT-SZ clusters

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